is the gas temperature, and using the laws of photoionized gas
described in great detail in [1]}.
Hence, our method ignores any explicit treatment of the radiation pressure
from the photon field of the central star.

This is correct for cool blue supergiant stars, while we neglect the
detailed position of the ionization front generated by the young
Wolf-Rayet stars, as well as its effects on the shell
instabilities [2]}.
